Towards Contextual S-BPM: Method and Case Study

Bonaldi, David; Totter, Alexandra; Pintér, Éva

doi:10.1007/978-3-642-23471-2_7

Cited by 4 publications

(7 citation statements)

References 3 publications

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“…Following our conclusions concerning the assessment of the background region (see Appendix B), we assume that the AME associated with the molecular cloud material can be modelled with a single component of spinning dust (Draine & Lazarian 1998). For this we use the Bonaldi et al (2007) model, a phenomenological model consisting of a parabola in logarithmic space (log(S ν )-log(ν)). The model is described by three free parameters: the slope at a frequency of 60 GHz, m 60 , which is a function of the width of the parabola, the central frequency, ν AME,peak , and the amplitude of the parabola, S AME,peak .…”

Section: Intensity Sed Modellingmentioning

confidence: 99%

QUIJOTE scientific results – III. Microwave spectrum of intensity and polarization in the Taurus Molecular Cloud complex and L1527

Poidevin

Rubiño-Martín

Dickinson

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present new intensity and polarization observations of the Taurus molecular cloud (TMC) region in the frequency range 10-20 GHz with the Multi-Frequency Instrument (MFI) mounted on the first telescope of the QUIJOTE experiment. From the combination of the QUIJOTE data with the WMAP 9-yr data release, the Planck second data release, the DIRBE maps and ancillary data, we detect an anomalous microwave emission (AME) component with flux density S AME,peak = 43.0 ± 7.9 Jy in the Taurus Molecular Cloud (TMC) and S AME,peak = 10.7 ± 2.7 Jy in the dark cloud nebula L1527, which is part of the TMC. In the TMC the diffuse AME emission peaks around a frequency of 19 GHz, compared with an emission peak about a frequency of 25 GHz in L1527. In the TMC, the best constraint on the level of AME polarization is obtained at the Planck channel of 28.4 GHz, with an upper limit π AME <4.2 % (95 % C. L.), which reduces to π AME <3.8 % (95 % C.L.) if the intensity of all the freefree, synchrotron and thermal dust components are negligible at this frequency. The same analysis in L1527 leads to π AME <5.3% (95 %C.L.), or π AME <4.5 % (95%C.L.) under the same assumption. We find that in the TMC and L1527 on average about 80% of the HII gas should be mixed with thermal dust. Our analysis shows how the QUIJOTE-MFI 10-20 GHz data provides key information to properly separate the synchrotron, free-free and AME components.

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Section: Intensity Sed Modellingmentioning

confidence: 99%

QUIJOTE scientific results – III. Microwave spectrum of intensity and polarization in the Taurus Molecular Cloud complex and L1527

Poidevin

Rubiño-Martín

Dickinson

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…In order to break possible degeneracies between the free-free and the synchrotron parameters in W44r, we set a flat prior on the emission measure EM < 1340 cm −6 pc, which comes from the upper bound of the EM estimate from the Alves et al (2012) map (see Table 4). Following Irfan et al (2015), for the spinning dust emission we resort to the phenomenological model proposed by Bonaldi et al (2007), consisting of a parabola in the logarithmic space (log(Sν )-logν) described by three parameters: its slope at 60 GHz, m60, which is associated with the width of the parabola, its central frequency, ν peak AME , and its amplitude, S peak AME . Finally, the thermal dust is modelled as a single-component modified blackbody curve, τ250(ν/1200 GHz) β d Bν (T d ), which depends on three parameters: the optical depth at 250 µm, τ250, the emissivity spectral index, β d , and the dust temperature T d .…”

Section: Sed Modellingmentioning

confidence: 99%

“…5. The solid line represents the best-fit AME model of Bonaldi et al (2007). The colour curves in the three panels represent the spinning dust models of Draine & Lazarian (1998) for six different physical environments (indicated in the legends of the centre and right pannels), normalised to the same amplitude as the solid curve.…”

Section: Re-evaluation Of the Intensity Sed Of W44mentioning

confidence: 99%

QUIJOTE scientific results – II. Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44

Génova-Santos

Rubiño-Martín

Peláez-Santos

et al. 2016

Mon. Not. R. Astron. Soc.

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We present Q-U-I JOint TEnerife (QUIJOTE) intensity and polarisation maps at 10 − 20 GHz covering a region along the Galactic plane 24 • ∼ < l ∼ < 45 • , |b| ∼ < 8 • . These maps result from 210 h of data, have a sensitivity in polarisation of ≈40 µK beam −1 and an angular resolution of ≈ 1 • . Our intensity data are crucial to confirm the presence of anomalous microwave emission (AME) towards the two molecular complexes W43 (22σ) and W47 (8σ). We also detect at high significance (6σ) AME associated with W44, the first clear detection of this emission towards a SNR. The new QUI-JOTE polarisation data, in combination with WMAP, are essential to: i) Determine the spectral index of the synchrotron emission in W44, β sync = −0.62 ± 0.03, in good agreement with the value inferred from the intensity spectrum once a free-free component is included in the fit. ii) Trace the change in the polarisation angle associated with Faraday rotation in the direction of W44 with rotation measure −404 ± 49 rad m −2 . And iii) set upper limits on the polarisation of W43 of Π AME < 0.39 per cent (95 per cent C.L.) from QUIJOTE 17 GHz, and < 0.22 per cent from WMAP 41 GHz data, which are the most stringent constraints ever obtained on the polarisation fraction of the AME. For typical physical conditions (grain temperature and magnetic field strengths), and in the case of perfect alignment between the grains and the magnetic field, the models of electric or magnetic dipole emissions predict higher polarisation fractions.

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“…The consultant documents these observations using notes, sketches and sometimes photos to facilitate the identification and documentation of problems or "disturbances" from the perspective of the worker. The detailed steps of contextual design are described in (Beyer and Holtzblatt 1998;Bonaldi et al 2011) and include:…”

Section: Designing Industrial Workplaces In a Subject-oriented Waymentioning

confidence: 99%

“…Prototyping results inform the (organizational and technical) implementation of desired solutions. An enrichment of S-BPM models with context information to be able to support contextual design has been presented in Bonaldi et al (2011). In the contextual design approach, this information is captured in five "work models" showing different aspects or dimensions of the work context (Beyer and Holtzblatt 1998;Holtzblatt and Beyer 2014).…”

Section: Designing Industrial Workplaces In a Subject-oriented Waymentioning

confidence: 99%

S-BPM’s Industrial Capabilities

Neubauer

Stary

Kannengiesser³

et al. 2016

S-BPM in the Production Industry

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S-BPM targets Business Process Management and has been applied in various business domains to model business processes and implement workflow support. This chapter investigates S-BPM's capabilities to support workplace and process design as well as process execution in production companies. Thereby, industrial capabilities of S-BPM are structured along the three dimensions of socio-technical systems which need to be considered for Industry 4.0 developments. Technological capabilities address the ability to integrate processes on different automation levels (planning, monitoring, real-time execution, etc.). Organizational capabilities discuss the potential of subject orientation for organizational development, and human capability development investigates how humans in production companies could be supported when involving them in workplace (re)design.

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Towards Contextual S-BPM: Method and Case Study

Cited by 4 publications

References 3 publications

QUIJOTE scientific results – III. Microwave spectrum of intensity and polarization in the Taurus Molecular Cloud complex and L1527

QUIJOTE scientific results – III. Microwave spectrum of intensity and polarization in the Taurus Molecular Cloud complex and L1527

QUIJOTE scientific results – II. Polarisation measurements of the microwave emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44

S-BPM’s Industrial Capabilities

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